Asteroseismology of beta Cephei and Be type stars

Abstract

The thesis focuses on the asteroseismology of main sequence B-type stars, particularly \(\beta\) Cephei and Be stars. Photometric observations of these stars were analysed in order to detect stellar oscillations. The photometric data analysed in this thesis were collected using the Solar Mass Ejection Imager (SMEI). The analysis initially focussed on known \(\beta\) Cephei stars, to refine information on previously detected frequencies and detect further oscillations. A survey was then conducted using data from the SMEI instrument to search for further \(\beta\) Cephei stars. The results from this survey were analysed, and individual stars were examined in more detail which may possibly be \(\beta\) Cephei like. Due to the long duration of light curves obtained with the SMEI instrument, stellar oscillations can be analysed for evidence of amplitude and phase change. This type of analysis was completed on two Be stars, Achernar and \(\zeta\) Oph, and significant amplitude changes in the oscillations of both of these stars were detected. There is evidence that the amplitude variations may be linked with the outburst events that occur on Be stars, and therefore this analysis may be used to help solve the puzzle of the Be phenomenon.

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